Asteroseismology using quadrupolar f-modes revisited: breaking of universal relationships in the slow hadron-quark conversion scenario

Abstract

In this work, we consider polar perturbations and we calculate the frequency and damping time of the quadrupolar fundamental f -mode of compact objects, constructed using a wide range of model-independent hybrid equations of state that include quark matter. We give special attention to the impact of the hadron-quark conversion speed that, in the slow case, gives rise to a branch of slow stable hybrid stars. Moreover, we study the validity of universal relationships proposed in the literature and find out that none of them remains valid when slow stable hybrid stars are taken into account. This fact could constrain the applicability of asteroseismology methods with fundamental modes designed to estimate the properties of pulsating compact objects. We hope that this result could be tested with the start up of the third-generation gravitational wave observatories, which might shed some light on the f -mode emission from compact objects.

13 pages, 13 figures. Comments are welcome

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• Probing hadron-quark phase transition in twin stars using $f$-modes
• Radial and Non-Radial Oscillations of Inverted Hybrid Stars
• Confronting new NICER mass-radius measurements with phase transition in dense matter and twin compact stars
• Assessing equation of state-independent relations for neutron stars with nonparametric models
• Towards a unified hadron-quark equation of state for neutron stars within the relativistic mean-field model
• Exploring Radial Oscillations in Slow Stable and Hybrid Neutron Stars
• How Neutron Star Observations Point Towards Exotic Matter: Existing Explanations and a Prospective Proposal
• Modification of the universal relation between mass, radius and nonradial $f$-mode oscillation in proto-neutron stars
• Systematic study of the morphology and length of slow stable hybrid star branches
• Classification of $g$-modes for neutron stars with a strong transition: Novel universal relation including slow stable hybrid stars
• Binding energy of compact stars and their non-radial oscillations